Properties of the KISS Green Pea Galaxies

Brunker, Samantha W.; Salzer, John J.; Janowiecki, Steven; Finn, Rose; Hélou, G.

doi:10.3847/1538-4357/ab9ec0

Cited by 23 publications

(27 citation statements)

References 77 publications

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“…These galaxies turned out to be much more than just an "interesting curiosity". They have low stellar masses (≈10 9 M e ), high specific star formation rates (≈10 −8 yr −1 ), small sizes (1 kpc, completely unresolved at ground-based resolution), and their optical spectra are characterized by extreme equivalent widths (EWs) in the [O III]λ5007 and Hα emission lines (e.g., Yang et al 2017b;Brunker et al 2020).…”

Section: Introductionmentioning

confidence: 99%

An Old Stellar Population or Diffuse Nebular Continuum Emission Discovered in Green Pea Galaxies

Clarke¹,

Scarlata²,

Mehta³

et al. 2021

ApJL

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We use new Hubble Space Telescope (HST) images of nine Green Pea galaxies (GPGs) to study their resolved structure and color. The choice of filters, F555W and F850LP, together with the redshift of the galaxies (z ∼ 0.25), minimizes the contribution of the nebular [O III] and Hα emission lines to the broadband images. While these galaxies are typically very blue in color, our analysis reveals that it is only the dominant stellar clusters that are blue. Each GPG does clearly show the presence of at least one bright and compact star-forming region, but these are invariably superimposed on a more extended and lower surface brightness emission. Moreover, the colors of the star-forming regions are on average bluer than those of the diffuse emission, reaching up to 0.6 magnitudes bluer. Assuming that the diffuse and compact components have constant and single-burst star formation histories, respectively, the observed colors imply that the diffuse components (possibly the host galaxy of the star formation episode) have, on average, old stellar ages (>1 Gyr), while the star clusters are younger than 500 Myr. While a redder stellar component is perhaps the most plausible explanation for these results, the limitations of our current data set lead us to examine possible alternative mechanisms, particularly recombination emission processes, which are unusually prominent in systems with such strong line emission. With the available data, however, it is not possible to distinguish between these two interpretations. A substantial presence of old stars would indicate that the mechanisms allowing large escape fractions in these local galaxies may be different from those at play during the reionization epoch.

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Section: Introductionmentioning

confidence: 99%

An Old Stellar Population or Diffuse Nebular Continuum Emission Discovered in Green Pea Galaxies

Clarke¹,

Scarlata²,

Mehta³

et al. 2021

ApJL

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“…One of these, Hα Dot 1021, was detected via strong [O III]λ5007 being located in our survey filter. This object has a spectrum similar to the Green Pea galaxies (Cardamone et al 2009;Brunker et al 2020). All of the remaining 12 Hα Dots with SDSS spectra are QSOs.…”

Section: 1 M Hα Dot Survey: Resultsmentioning

confidence: 87%

“…The nature of our selection method results in catalogs of strong-lined objects that identify very specific types of star-forming and active galaxies detected via a number of different emission lines. In particular, the Hα Dots detected via the Hα line are all dwarf starforming galaxies (including many blue compact dwarf (BCD) galaxies) or outlying H II regions in nearby spiral galaxies, while those detected via the [O III]λ5007 line are typically Green Pea galaxies (e.g., Cardamone et al 2009;Brunker et al 2020) or Seyfert 2 galaxies (Salzer et al 2020). The Hα Dots survey also detects high redshift QSOs via one of several UV emission lines (e.g., Mg II λ2798, C IV λ1549 or Lyα).…”

Section: Introductionmentioning

confidence: 99%

The H$α$ Dots Survey. IV. A Fourth List of Faint Emission-Line Objects

Watkins,

Salzer,

Van Sistine

et al. 2021

Preprint

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We present the fourth catalog of serendipitously discovered compact extragalactic emission-line sources -Hα Dots. A total of 454 newly discovered objects are included in the current survey list. These objects have been detected in searches of moderately deep narrow-band images acquired for the ALFALFA Hα project (Van Sistine et al. 2016). The catalog of Hα Dots presented in the current paper was derived from searches carried out using ALFALFA Hα images obtained with the KPNO 2.1 m telescope. This results in a substantially deeper sample of Dots compared to our previous lists, which were all discovered in images taken with the WIYN 0.9 m telescope. The median R-band magnitude of the current catalog is 21.59, more than 1.6 magnitudes fainter than the median for the 0.9 m sample (factor of 4.4× fainter). Likewise, the median emission-line flux of the detected sources is a factor of 4.3× fainter. The line-flux completeness limit of the current sample is approximately 3 × 10 −16 erg s −1 cm −2 . We present accurate coordinates, apparent magnitudes and narrow-band line fluxes for each object in the sample. Unlike our previous lists of Hα Dots, the current sample does not include follow-up spectroscopy.

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“…Blueberry galaxies at z < 0.05 are the lowest mass young starburst galaxies (Yang et al 2017) where the [OIII]λ5007 emission line is located within the g−band and the Hα emission line is located within the r−band. Purple Grape galaxies (Izotov et al 2011;Brunker et al 2020) where either that the [OIII]λ5007 emission line is located in the i−band at z > 0.36 and the UV continuum is redshifted to the g−band, or the [OIII]λ5007 is located in the g-band and the Hα emission line is located in the i−band (0.112 < z < 0.36).…”

Section: Introductionmentioning

confidence: 99%

Strong [OIII]λ5007 emission line compact galaxies in LAMOST DR9: Blueberries, Green Peas and Purple Grapes

Liu,

Luo,

Yang

et al. 2022

Preprint

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Green Pea and Blueberry galaxies are well-known for their compact size, low mass, strong emission lines and analogs to high-z Lyα emitting galaxies. In this study, 1547 strong [OIII]λ5007 emission line compact galaxies with 1694 spectra are selected from LAMOST DR9 at the redshift range from 0.0 to 0.59. According to the redshift distribution, these samples can be separated into three groups: Blueberries, Green Peas and Purple Grapes. Optical [MgII]λ2800 line feature, BPT diagram, multiwavelength SED fitting, MIR color, and MIR variability are deployed to identify 23 AGN candidates from these samples, which are excluded for the following SFR discussions. We perform the multiwavelength SED fitting with GALEX UV and WISE MIR data. Color excess from Balmer decrement shows these strong [OIII]λ5007 emission line compact galaxies are not highly reddened. The stellar mass of the galaxies is obtained by fitting LAMOST calibrated spectra with the emission lines masked. We find that the SFR is increasing with the increase of redshift, while for the sources within the same redshift bin, the SFR increases with mass with a similar slope as the SFMS. These samples have a median metallicity of 12+log(O/H) of 8.10. The metallicity increases with mass, and all the sources are below the mass-metallicity relation. The direct-derived T e -based metallicity from the [OIII]λ4363 line agrees with the empirical N2-based empirical gas-phase metallicity. Moreover, these compact strong [OIII]λ5007 are mostly in a less dense environment.

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Properties of the KISS Green Pea Galaxies

Cited by 23 publications

References 77 publications

An Old Stellar Population or Diffuse Nebular Continuum Emission Discovered in Green Pea Galaxies

An Old Stellar Population or Diffuse Nebular Continuum Emission Discovered in Green Pea Galaxies

The H$α$ Dots Survey. IV. A Fourth List of Faint Emission-Line Objects

Strong [OIII]λ5007 emission line compact galaxies in LAMOST DR9: Blueberries, Green Peas and Purple Grapes

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